High Energy Astrophysical Phenomena (astro-ph.HE)
Thu, 22 Jun 2023
1.Possible contribution of X-ray binary jets to the Galactic cosmic ray and neutrino flux
Authors:Dimitrios Kantzas, Sera Markoff, Alex J. Cooper, Daniele Gaggero, Maria Petropoulou, Pedro De La Torre Luque
Abstract: For over a century, the identification of high-energy cosmic ray (CR) sources remains an open question. For Galactic CRs with energy up to $10^{15}$ eV, supernova remnants (SNRs) have traditionally been thought the main candidate source. However, recent TeV gamma-ray observations have questioned the SNR paradigm. Propagating CRs are deflected by the Galactic magnetic field, hence, gamma-rays and neutrinos produced via inelastic hadronic interactions are the only means for unveiling the CR sources. In this work, we study the gamma-ray and neutrino emission produced by CRs accelerated inside Galactic jets of stellar-mass black holes in X-ray binaries (BHXBs). We calculate the intrinsic neutrino emission of two prototypical BHXBs, Cygnus X-1 and GX 339-4, for which we have high-quality, quasi-simultaneous multiwavelength spectra. Based on these prototypical sources, we discuss the likelihood of the 35 known Galactic BHXBs to be efficient CR accelerators. Moreover, we estimate the potential contribution to the CR spectrum of a viable population of BHXBs that reside in the Galactic plane. When these BHXBs go into outburst, they may accelerate particles up to 100s of TeV that contribute to the diffuse gamma-ray and neutrino spectra while propagating in the Galactic medium. Using HERMES, an open-source code that calculates the hadronic processes along the line of sight, we discuss the contribution of BHXBs to the diffuse gamma-ray and neutrino fluxes, and compare these to their intrinsic gamma-ray and neutrino emissions. Finally, we discuss the contribution of BHXBs to the observed spectrum of Galactic CRs.
2.Constraints on the cosmological parameters with three-parameter correlation of Gamma-ray bursts
Authors:Jia-Lun Li, Yu-Peng Yang, Shuang-Xi Yi, Jian-Ping Hu, Fa-Yin Wang, Yan-Kun Qu
Abstract: As one of the most energetic and brightest events, gamma-ray bursts (GRBs) can be treated as a promising probe of the high-redshift universe. Similar to type Ia supernovae (SNe Ia), GRBs with same physical origin could be treated as standard candles. We select GRB samples with the same physical origin, which are divided into two groups. One group is consisted of 31 GRBs with a plateau phase feature of a constant luminosity followed by a decay index of about -2 in the X-ray afterglow light curves, and the other has 50 GRBs with a shallow decay phase in the optical light curves. For the selected GRB samples, we confirm that there is a tight correlation between the plateau luminosity $L_0$, the end time of plateau $t_b$ and the isotropic energy release $E_{\gamma,iso}$. We also find that the $L_0-t_b-E_{\gamma,iso}$ correlation is insensitive to the cosmological parameters and no valid limitations on the cosmological parameters can be obtained using this correlation. We explore a new three-parameter correlation $L_0$, $t_b$, and the spectral peak energy in the rest frame $E_{p,i}$ ($L_0-t_b-E_{p,i}$), and find that this correlation can be used as a standard candle to constrain the cosmological parameters. By employing the optical sample only, we find the constraints of $\Omega_m = 0.697_{-0.278}^{+0.402}(1\sigma)$ for a flat $\Lambda$CDM model. For the non-flat $\Lambda$CDM model, the best-fitting results are $\Omega_m = 0.713_{-0.278}^{+0.346}$, $\Omega_{\Lambda} = 0.981_{-0.580}^{+0.379}(1\sigma)$. For the combination of the X-ray and optical smaples, we find $\Omega_m = 0.313_{-0.125}^{+0.179}(1\sigma)$ for a flat $\Lambda$CDM model, and $\Omega_m = 0.344_{-0.112}^{+0.176}$, $\Omega_{\Lambda} = 0.770_{-0.416}^{+0.366}(1\sigma)$ for a non-flat $\Lambda$CDM model.
3.No plateau observed in late-time near-infrared observations of the underluminous Type Ia supernova 2021qvv
Authors:O. Graur, E. Padilla Gonzalez, J. Burke, M. Deckers, S. W. Jha, L. Galbany, E. Karamenhmetoglu, M. D. Stritzinger, K. Maguire, D. A. Howell, R. Fisher, A. G. Fullard, R. Handberg, G. Hosseinzadeh, W. E. Kerzendorf, C. McCully, M. Newsome, A. Rest, A. G. Riess, I. R. Seitenzahl, M. M. Shara, K. J. Shen, G. Terreran, D. R. Zurek
Abstract: Near-infrared (NIR) observations of normal Type Ia supernovae (SNe Ia) obtained between 150 to 500 d past maximum light reveal the existence of an extended plateau. Here, we present observations of the underluminous, 1991bg-like SN 2021qvv. Early, ground-based optical and NIR observations show that SN 2021qvv is similar to SN 2006mr, making it one of the dimmest, fastest-evolving 1991bg-like SNe to date. Late-time (170-250 d) Hubble Space Telescope observations of SN 2021qvv reveal no sign of a plateau. An extrapolation of these observations backwards to earlier-phase NIR observations of SN 2006mr suggests the complete absence of a NIR plateau, at least out to 250 d. This absence may be due to the lower temperatures of the ejecta of 1991bg-like SNe, relative to normal SNe Ia, which might preclude their becoming fluorescent and shifting ultraviolet light into the NIR. This suggestion can be tested by acquiring NIR imaging of a sample of 1991bg-like SNe that covers the entire range from slowly-evolving to fast-evolving events ($0.2 \lesssim s_\mathrm{BV} \lesssim 0.6$). A detection of the NIR plateau in slower-evolving, hotter 1991bg-like SNe would provide further evidence that these SNe exist along a continuum with normal SNe Ia. Theoretical progenitor and explosion scenarios would then have to match the observed properties of both SN Ia subtypes.
4.Type Ia Supernova Nucleosynthesis: Metallicity-Dependent Yields
Authors:James D Keegans, Marco Pignatari, Richard J Stancliffe, Claudia Travaglio, Samuel Jones, Brad K Gibson, Dean M Townsley, Broxton J Miles, Ken J Shen, Gareth Few
Abstract: Type Ia supernova explosions (SNIa) are fundamental sources of elements for the chemical evolution of galaxies. They efficiently produce intermediate-mass (with Z between 11 and 20) and iron group elements - for example, about 70% of the solar iron is expected to be made by SNIa. In this work, we calculate complete abundance yields for 39 models of SNIa explosions, based on three progenitors - a 1.4M deflagration detonation model, a 1.0 double detonation model and a 0.8 M double detonation model - and 13 metallicities, with 22Ne mass fractions of 0, 1x10-7, 1x10-6, 1x10-5, 1x10-4, 1x10-3, 2x10-3, 5x10-3, 1x10-2, 1.4x10-2, 5x10-2, and 0.1 respectively. Nucleosynthesis calculations are done using the NuGrid suite of codes, using a consistent nuclear reaction network between the models. Complete tables with yields and production factors are provided online at Zenodo: Yields. We discuss the main properties of our yields in the light of the present understanding of SNIa nucleosynthesis, depending on different progenitor mass and composition. Finally, we compare our results with a number of relevant models from the literature.
5.Observations of the Crab Nebula and Pulsar with the Large-Sized Telescope Prototype of the Cherenkov Telescope Array
Authors:CTA-LST Project Institute for Cosmic Ray Research, University of Tokyo, Chiba, Japan, : Institute for Cosmic Ray Research, University of Tokyo, Chiba, Japan, S. Abe Institute for Cosmic Ray Research, University of Tokyo, Chiba, Japan, A. Aguasca-Cabot Departament de Física Quàntica i Astrofísica, Institut de Ciències del Cosmos, Universitat de Barcelona, IEEC-UB, Barcelona, Spain, I. Agudo Instituto de Astrofísica de Andalucía-CSIC, Glorieta de la Astronomía, Granada, Spain, N. Alvarez Crespo IPARCOS-UCM, Instituto de Física de Partículas y del Cosmos, and EMFTEL Department, Universidad Complutense de Madrid, Madrid, Spain, L. A. Antonelli INAF - Osservatorio Astronomico di Roma, Monteporzio Catone, Italy, C. Aramo INFN Sezione di Napoli, Napoli, Italy, A. Arbet-Engels Max-Planck-Institut für Physik, München, Germany, M. Artero Institut de Fisica d'Altes Energies, K. Asano Institute for Cosmic Ray Research, University of Tokyo, Chiba, Japan, P. Aubert Univ. Savoie Mont Blanc, CNRS, Laboratoire d'Annecy de Physique des Particules - IN2P3, Annecy, France, A. Baktash Universität Hamburg, Institut für Experimentalphysik, Hamburg, Germany, A. Bamba Graduate School of Science, University of Tokyo, Tokyo, Japan, A. Baquero Larriva IPARCOS-UCM, Instituto de Física de Partículas y del Cosmos, and EMFTEL Department, Universidad Complutense de Madrid, Madrid, Spain Faculty of Science and Technology, Universidad del Azuay, Cuenca, Ecuador, L. Baroncelli INAF - Osservatorio di Astrofisica e Scienza dello spazio di Bologna, Bologna, Italy, U. Barres de Almeida Centro Brasileiro de Pesquisas Físicas, Rio de Janeiro, Brazil, J. A. Barrio IPARCOS-UCM, Instituto de Física de Partículas y del Cosmos, and EMFTEL Department, Universidad Complutense de Madrid, Madrid, Spain, I. Batkovic INFN Sezione di Padova and Università degli Studi di Padova, Padova, Italy, J. Baxter Institute for Cosmic Ray Research, University of Tokyo, Chiba, Japan, J. Becerra González Instituto de Astrofísica de Canarias and Departamento de Astrofísica, Universidad de La Laguna, Tenerife, Spain, E. Bernardini INFN Sezione di Padova and Università degli Studi di Padova, Padova, Italy, M. I. Bernardos Instituto de Astrofísica de Andalucía-CSIC, Glorieta de la Astronomía, Granada, Spain, J. Bernete Medrano CIEMAT, Avda. Complutense Madrid, Spain, A. Berti Max-Planck-Institut für Physik, München, Germany, P. Bhattacharjee Univ. Savoie Mont Blanc, CNRS, Laboratoire d'Annecy de Physique des Particules - IN2P3, Annecy, France, N. Biederbeck Department of Physics, TU Dortmund University, Dortmund, Germany, C. Bigongiari INAF - Osservatorio Astronomico di Roma, Monteporzio Catone, Italy, E. Bissaldi INFN Sezione di Bari and Politecnico di Bari, Bari, Italy, O. Blanch Institut de Fisica d'Altes Energies, P. Bordas Departament de Física Quàntica i Astrofísica, Institut de Ciències del Cosmos, Universitat de Barcelona, IEEC-UB, Barcelona, Spain, A. Bulgarelli INAF - Osservatorio di Astrofisica e Scienza dello spazio di Bologna, Bologna, Italy, I. Burelli INFN Sezione di Trieste and Università degli studi di Udine, Udine, Italy, M. Buscemi INFN Sezione di Catania, Catania, Italy, M. Cardillo INAF - Istituto di Astrofisica e Planetologia Spaziali, S. Caroff Univ. Savoie Mont Blanc, CNRS, Laboratoire d'Annecy de Physique des Particules - IN2P3, Annecy, France, A. Carosi INAF - Osservatorio Astronomico di Roma, Monteporzio Catone, Italy, F. Cassol Aix Marseille Univ, CNRS/IN2P3, CPPM, Marseille, France, D. Cauz INFN Sezione di Trieste and Università degli studi di Udine, Udine, Italy, G. Ceribella Institute for Cosmic Ray Research, University of Tokyo, Chiba, Japan, Y. Chai Max-Planck-Institut für Physik, München, Germany, K. Cheng Institute for Cosmic Ray Research, University of Tokyo, Chiba, Japan, A. Chiavassa INFN Sezione di Torino, Torino, Italy, M. Chikawa Institute for Cosmic Ray Research, University of Tokyo, Chiba, Japan, L. Chytka Palacky University Olomouc, Faculty of Science, Olomouc, Czech Republic, A. Cifuentes CIEMAT, Avda. Complutense Madrid, Spain, J. L. Contreras IPARCOS-UCM, Instituto de Física de Partículas y del Cosmos, and EMFTEL Department, Universidad Complutense de Madrid, Madrid, Spain, J. Cortina CIEMAT, Avda. Complutense Madrid, Spain, H. Costantini Aix Marseille Univ, CNRS/IN2P3, CPPM, Marseille, France, G. D'Amico Department of Physics and Technology, University of Bergen, Bergen, Norway, M. Dalchenko University of Geneva - Département de physique nucléaire et corpusculaire, Genève, Switzerland, A. De Angelis INFN Sezione di Padova and Università degli Studi di Padova, Padova, Italy, M. de Bony de Lavergne Univ. Savoie Mont Blanc, CNRS, Laboratoire d'Annecy de Physique des Particules - IN2P3, Annecy, France, B. De Lotto INFN Sezione di Trieste and Università degli studi di Udine, Udine, Italy, R. de Menezes INFN Sezione di Torino, Torino, Italy, G. Deleglise Univ. Savoie Mont Blanc, CNRS, Laboratoire d'Annecy de Physique des Particules - IN2P3, Annecy, France, C. Delgado CIEMAT, Avda. Complutense Madrid, Spain, J. Delgado Mengual Port d'Informació Científica, Bellaterrra, D. della Volpe University of Geneva - Département de physique nucléaire et corpusculaire, Genève, Switzerland, M. Dellaiera Univ. Savoie Mont Blanc, CNRS, Laboratoire d'Annecy de Physique des Particules - IN2P3, Annecy, France, D. Depaoli INFN Sezione di Torino, Torino, Italy, A. Di Piano INAF - Osservatorio di Astrofisica e Scienza dello spazio di Bologna, Bologna, Italy, F. Di Pierro INFN Sezione di Torino, Torino, Italy, R. Di Tria INFN Sezione di Bari and Università di Bari, Bari, Italy, L. Di Venere INFN Sezione di Bari and Università di Bari, Bari, Italy, C. Díaz CIEMAT, Avda. Complutense Madrid, Spain, R. M. Dominik Department of Physics, TU Dortmund University, Dortmund, Germany, D. Dominis Prester University of Rijeka, Department of Physics, Rijeka, Croatia, A. Donini Institut de Fisica d'Altes Energies, D. Dorner Institute for Theoretical Physics and Astrophysics, Universität Würzburg, Campus Hubland Nord, Würzburg, Germany, M. Doro INFN Sezione di Padova and Università degli Studi di Padova, Padova, Italy, D. Elsässer Department of Physics, TU Dortmund University, Dortmund, Germany, G. Emery University of Geneva - Département de physique nucléaire et corpusculaire, Genève, Switzerland, J. Escudero Instituto de Astrofísica de Andalucía-CSIC, Glorieta de la Astronomía, Granada, Spain, V. Fallah Ramazani Institut für Theoretische Physik, Lehrstuhl IV: Plasma-Astroteilchenphysik, Ruhr-Universität Bochum, Bochum, Germany, G. Ferrara INFN Sezione di Catania, Catania, Italy, A. Fiasson Univ. Savoie Mont Blanc, CNRS, Laboratoire d'Annecy de Physique des Particules - IN2P3, Annecy, France ILANCE, CNRS - University of Tokyo International Research Laboratory, Kashiwa, Chiba, Japan, L. Freixas Coromina CIEMAT, Avda. Complutense Madrid, Spain, S. Fröse Department of Physics, TU Dortmund University, Dortmund, Germany, S. Fukami Institute for Cosmic Ray Research, University of Tokyo, Chiba, Japan, Y. Fukazawa Physics Program, Graduate School of Advanced Science and Engineering, Hiroshima University, Hiroshima, Japan, E. Garcia Univ. Savoie Mont Blanc, CNRS, Laboratoire d'Annecy de Physique des Particules - IN2P3, Annecy, France, R. Garcia López Instituto de Astrofísica de Canarias and Departamento de Astrofísica, Universidad de La Laguna, Tenerife, Spain, D. Gasparrini INFN Sezione di Roma Tor Vergata, Rome, Italy, F. Geyer Department of Physics, TU Dortmund University, Dortmund, Germany, J. Giesbrecht Paiva Centro Brasileiro de Pesquisas Físicas, Rio de Janeiro, Brazil, N. Giglietto INFN Sezione di Bari and Politecnico di Bari, Bari, Italy, F. Giordano INFN Sezione di Bari and Università di Bari, Bari, Italy, E. Giro INFN Sezione di Padova and Università degli Studi di Padova, Padova, Italy, P. Gliwny Faculty of Physics and Applied Informatics, University of Lodz, Lodz, Poland, N. Godinovic University of Split, FESB, Split, Croatia, R. Grau Institut de Fisica d'Altes Energies, J. Green Max-Planck-Institut für Physik, München, Germany, D. Green Max-Planck-Institut für Physik, München, Germany, S. Gunji Department of Physics, Yamagata University, Yamagata, Yamagata, Japan, J. Hackfeld Institut für Theoretische Physik, Lehrstuhl IV: Plasma-Astroteilchenphysik, Ruhr-Universität Bochum, Bochum, Germany, D. Hadasch Institute for Cosmic Ray Research, University of Tokyo, Chiba, Japan, A. Hahn Max-Planck-Institut für Physik, München, Germany, K. Hashiyama Institute for Cosmic Ray Research, University of Tokyo, Chiba, Japan, T. Hassan CIEMAT, Avda. Complutense Madrid, Spain, K. Hayashi Tohoku University, Astronomical Institute, Aobaku, Sendai 980-8578, Japan, L. Heckmann Max-Planck-Institut für Physik, München, Germany, M. Heller University of Geneva - Département de physique nucléaire et corpusculaire, Genève, Switzerland, J. Herrera Llorente Instituto de Astrofísica de Canarias and Departamento de Astrofísica, Universidad de La Laguna, Tenerife, Spain, K. Hirotani Institute for Cosmic Ray Research, University of Tokyo, Chiba, Japan, D. Hoffmann Aix Marseille Univ, CNRS/IN2P3, CPPM, Marseille, France, D. Horns Universität Hamburg, Institut für Experimentalphysik, Hamburg, Germany, J. Houles Aix Marseille Univ, CNRS/IN2P3, CPPM, Marseille, France, M. Hrabovsky Palacky University Olomouc, Faculty of Science, Olomouc, Czech Republic, D. Hrupec Josip Juraj Strossmayer University of Osijek, Department of Physics, Osijek, Croatia, D. Hui Institute for Cosmic Ray Research, University of Tokyo, Chiba, Japan, M. Hütten Institute for Cosmic Ray Research, University of Tokyo, Chiba, Japan, R. Imazawa Physics Program, Graduate School of Advanced Science and Engineering, Hiroshima University, Hiroshima, Japan, T. Inada Institute for Cosmic Ray Research, University of Tokyo, Chiba, Japan, Y. Inome Institute for Cosmic Ray Research, University of Tokyo, Chiba, Japan, K. Ioka Kitashirakawa Oiwakecho, Sakyo Ward, Kyoto, Japan, M. Iori INFN Sezione di Roma La Sapienza, Rome, Italy, K. Ishio Faculty of Physics and Applied Informatics, University of Lodz, Lodz, Poland, Y. Iwamura Institute for Cosmic Ray Research, University of Tokyo, Chiba, Japan, M. Jacquemont Univ. Savoie Mont Blanc, CNRS, Laboratoire d'Annecy de Physique des Particules - IN2P3, Annecy, France, I. Jimenez Martinez CIEMAT, Avda. Complutense Madrid, Spain, J. Jurysek Department of Astronomy, University of Geneva, Versoix, Switzerland, M. Kagaya Institute for Cosmic Ray Research, University of Tokyo, Chiba, Japan, V. Karas Astronomical Institute of the Czech Academy of Sciences, Prague, Czech Republic, H. Katagiri Faculty of Science, Ibaraki University, Ibaraki, Japan, J. Kataoka Faculty of Science and Engineering, Waseda University, Shinjuku, Tokyo, Japan, D. Kerszberg Institut de Fisica d'Altes Energies, Y. Kobayashi Institute for Cosmic Ray Research, University of Tokyo, Chiba, Japan, A. Kong Institute for Cosmic Ray Research, University of Tokyo, Chiba, Japan, H. Kubo Institute for Cosmic Ray Research, University of Tokyo, Chiba, Japan, J. Kushida Department of Physics, Tokai University, Kanagawa, Japan, M. Lainez IPARCOS-UCM, Instituto de Física de Partículas y del Cosmos, and EMFTEL Department, Universidad Complutense de Madrid, Madrid, Spain, G. Lamanna Univ. Savoie Mont Blanc, CNRS, Laboratoire d'Annecy de Physique des Particules - IN2P3, Annecy, France, A. Lamastra INAF - Osservatorio Astronomico di Roma, Monteporzio Catone, Italy, T. Le Flour Univ. Savoie Mont Blanc, CNRS, Laboratoire d'Annecy de Physique des Particules - IN2P3, Annecy, France, M. Linhoff Department of Physics, TU Dortmund University, Dortmund, Germany, F. Longo INFN Sezione di Trieste and Università degli Studi di Trieste, Trieste, Italy, R. López-Coto Instituto de Astrofísica de Andalucía-CSIC, Glorieta de la Astronomía, Granada, Spain, M. López-Moya IPARCOS-UCM, Instituto de Física de Partículas y del Cosmos, and EMFTEL Department, Universidad Complutense de Madrid, Madrid, Spain, A. López-Oramas Instituto de Astrofísica de Canarias and Departamento de Astrofísica, Universidad de La Laguna, Tenerife, Spain, S. Loporchio INFN Sezione di Bari and Università di Bari, Bari, Italy, A. Lorini INFN and Università degli Studi di Siena, Dipartimento di Scienze Fisiche, della Terra e dell'Ambiente, P. L. Luque-Escamilla Escuela Politécnica Superior de Jaén, Universidad de Jaén, Campus Las Lagunillas, Jaén, Spain, P. Majumdar Institute for Cosmic Ray Research, University of Tokyo, Chiba, Japan Saha Institute of Nuclear Physics, Bidhannagar, India, M. Makariev Institute for Nuclear Research and Nuclear Energy, Bulgarian Academy of Sciences, Sofia, Bulgaria, D. Mandat FZU - Institute of Physics of the Czech Academy of Sciences, Praha, Czech Republic, M. Manganaro University of Rijeka, Department of Physics, Rijeka, Croatia, G. Manicò INFN Sezione di Catania, Catania, Italy, K. Mannheim Institute for Theoretical Physics and Astrophysics, Universität Würzburg, Campus Hubland Nord, Würzburg, Germany, M. Mariotti INFN Sezione di Padova and Università degli Studi di Padova, Padova, Italy, P. Marquez Institut de Fisica d'Altes Energies, G. Marsella INFN Sezione di Catania, Catania, Italy Dipartimento di Fisica e Chimica 'E. Segrè' Università degli Studi di Palermo, Palermo, J. Martí Escuela Politécnica Superior de Jaén, Universidad de Jaén, Campus Las Lagunillas, Jaén, Spain, O. Martinez Grupo de Electronica, Universidad Complutense de Madrid, Av. Complutense s/n, 28040 Madrid, Spain, G. Martínez CIEMAT, Avda. Complutense Madrid, Spain, M. Martínez Institut de Fisica d'Altes Energies, P. Marusevec Department of Applied Physics, University of Zagreb, Zagreb, Croatia, A. Mas-Aguilar IPARCOS-UCM, Instituto de Física de Partículas y del Cosmos, and EMFTEL Department, Universidad Complutense de Madrid, Madrid, Spain, G. Maurin Univ. Savoie Mont Blanc, CNRS, Laboratoire d'Annecy de Physique des Particules - IN2P3, Annecy, France, D. Mazin Institute for Cosmic Ray Research, University of Tokyo, Chiba, Japan Max-Planck-Institut für Physik, München, Germany, E. Mestre Guillen Institute of Space Sciences, S. Micanovic University of Rijeka, Department of Physics, Rijeka, Croatia, D. Miceli INFN Sezione di Padova and Università degli Studi di Padova, Padova, Italy, T. Miener IPARCOS-UCM, Instituto de Física de Partículas y del Cosmos, and EMFTEL Department, Universidad Complutense de Madrid, Madrid, Spain, J. M. Miranda Grupo de Electronica, Universidad Complutense de Madrid, Av. Complutense s/n, 28040 Madrid, Spain, R. Mirzoyan Max-Planck-Institut für Physik, München, Germany, T. Mizuno Hiroshima Astrophysical Science Center, Hiroshima University, Hiroshima, Japan, M. Molero Gonzalez Instituto de Astrofísica de Canarias and Departamento de Astrofísica, Universidad de La Laguna, Tenerife, Spain, E. Molina Departament de Física Quàntica i Astrofísica, Institut de Ciències del Cosmos, Universitat de Barcelona, IEEC-UB, Barcelona, Spain, T. Montaruli University of Geneva - Département de physique nucléaire et corpusculaire, Genève, Switzerland, I. Monteiro Univ. Savoie Mont Blanc, CNRS, Laboratoire d'Annecy de Physique des Particules - IN2P3, Annecy, France, A. Moralejo Institut de Fisica d'Altes Energies, D. Morcuende IPARCOS-UCM, Instituto de Física de Partículas y del Cosmos, and EMFTEL Department, Universidad Complutense de Madrid, Madrid, Spain, A. Morselli INFN Sezione di Roma Tor Vergata, Rome, Italy, K. Mrakovcic University of Rijeka, Department of Physics, Rijeka, Croatia, K. Murase Institute for Cosmic Ray Research, University of Tokyo, Chiba, Japan, A. Nagai University of Geneva - Département de physique nucléaire et corpusculaire, Genève, Switzerland, T. Nakamori Department of Physics, Yamagata University, Yamagata, Yamagata, Japan, L. Nickel Department of Physics, TU Dortmund University, Dortmund, Germany, M. Nievas Instituto de Astrofísica de Canarias and Departamento de Astrofísica, Universidad de La Laguna, Tenerife, Spain, K. Nishijima Department of Physics, Tokai University, Kanagawa, Japan, K. Noda Institute for Cosmic Ray Research, University of Tokyo, Chiba, Japan, D. Nosek Charles University, Institute of Particle and Nuclear Physics, Prague, Czech Republic, S. Nozaki Max-Planck-Institut für Physik, München, Germany, M. Ohishi Institute for Cosmic Ray Research, University of Tokyo, Chiba, Japan, Y. Ohtani Institute for Cosmic Ray Research, University of Tokyo, Chiba, Japan, N. Okazaki Institute for Cosmic Ray Research, University of Tokyo, Chiba, Japan, A. Okumura Institute for Space-Earth Environmental Research, Nagoya University, Nagoya, Japan Kobayashi-Maskawa Institute, R. Orito Graduate School of Technology, Industrial and Social Sciences, Tokushima University, Tokushima, Japan, J. Otero-Santos Instituto de Astrofísica de Canarias and Departamento de Astrofísica, Universidad de La Laguna, Tenerife, Spain, M. Palatiello INFN Sezione di Trieste and Università degli studi di Udine, Udine, Italy, D. Paneque Max-Planck-Institut für Physik, München, Germany, F. R. Pantaleo INFN Sezione di Bari and Politecnico di Bari, Bari, Italy, R. Paoletti INFN and Università degli Studi di Siena, Dipartimento di Scienze Fisiche, della Terra e dell'Ambiente, J. M. Paredes Departament de Física Quàntica i Astrofísica, Institut de Ciències del Cosmos, Universitat de Barcelona, IEEC-UB, Barcelona, Spain, L. Pavletić University of Rijeka, Department of Physics, Rijeka, Croatia, M. Pech FZU - Institute of Physics of the Czech Academy of Sciences, Praha, Czech Republic, M. Pecimotika University of Rijeka, Department of Physics, Rijeka, Croatia, A. Pérez IPARCOS-UCM, Instituto de Física de Partículas y del Cosmos, and EMFTEL Department, Universidad Complutense de Madrid, Madrid, Spain, E. Pietropaolo INFN Dipartimento di Scienze Fisiche e Chimiche - Università degli Studi dell'Aquila and Gran Sasso Science Institute, L'Aquila, Italy, G. Pirola Max-Planck-Institut für Physik, München, Germany, C. Plard Univ. Savoie Mont Blanc, CNRS, Laboratoire d'Annecy de Physique des Particules - IN2P3, Annecy, France, F. Podobnik INFN and Università degli Studi di Siena, Dipartimento di Scienze Fisiche, della Terra e dell'Ambiente, V. Poireau Univ. Savoie Mont Blanc, CNRS, Laboratoire d'Annecy de Physique des Particules - IN2P3, Annecy, France, M. Polo CIEMAT, Avda. Complutense Madrid, Spain, E. Pons Univ. Savoie Mont Blanc, CNRS, Laboratoire d'Annecy de Physique des Particules - IN2P3, Annecy, France, E. Prandini INFN Sezione di Padova and Università degli Studi di Padova, Padova, Italy, J. Prast Univ. Savoie Mont Blanc, CNRS, Laboratoire d'Annecy de Physique des Particules - IN2P3, Annecy, France, G. Principe INFN Sezione di Trieste and Università degli Studi di Trieste, Trieste, Italy, C. Priyadarshi Institut de Fisica d'Altes Energies, M. Prouza FZU - Institute of Physics of the Czech Academy of Sciences, Praha, Czech Republic, R. Rando INFN Sezione di Padova and Università degli Studi di Padova, Padova, Italy, W. Rhode Department of Physics, TU Dortmund University, Dortmund, Germany, M. Ribó Departament de Física Quàntica i Astrofísica, Institut de Ciències del Cosmos, Universitat de Barcelona, IEEC-UB, Barcelona, Spain, V. Rizi INFN Dipartimento di Scienze Fisiche e Chimiche - Università degli Studi dell'Aquila and Gran Sasso Science Institute, L'Aquila, Italy, G. Rodriguez Fernandez INFN Sezione di Roma Tor Vergata, Rome, Italy, T. Saito Institute for Cosmic Ray Research, University of Tokyo, Chiba, Japan, S. Sakurai Institute for Cosmic Ray Research, University of Tokyo, Chiba, Japan, D. A. Sanchez Univ. Savoie Mont Blanc, CNRS, Laboratoire d'Annecy de Physique des Particules - IN2P3, Annecy, France, T. Šarić University of Split, FESB, Split, Croatia, F. G. Saturni INAF - Osservatorio Astronomico di Roma, Monteporzio Catone, Italy, B. Schleicher Institute for Theoretical Physics and Astrophysics, Universität Würzburg, Campus Hubland Nord, Würzburg, Germany, F. Schmuckermaier Max-Planck-Institut für Physik, München, Germany, J. L. Schubert Department of Physics, TU Dortmund University, Dortmund, Germany, F. Schussler IRFU, CEA, Université Paris-Saclay, Gif-sur-Yvette, France, T. Schweizer Max-Planck-Institut für Physik, München, Germany, M. Seglar Arroyo Univ. Savoie Mont Blanc, CNRS, Laboratoire d'Annecy de Physique des Particules - IN2P3, Annecy, France, J. Sitarek Faculty of Physics and Applied Informatics, University of Lodz, Lodz, Poland, V. Sliusar Department of Astronomy, University of Geneva, Versoix, Switzerland, A. Spolon INFN Sezione di Padova and Università degli Studi di Padova, Padova, Italy, J. Strišković Josip Juraj Strossmayer University of Osijek, Department of Physics, Osijek, Croatia, M. Strzys Institute for Cosmic Ray Research, University of Tokyo, Chiba, Japan, Y. Suda Physics Program, Graduate School of Advanced Science and Engineering, Hiroshima University, Hiroshima, Japan, Y. Sunada Graduate School of Science and Engineering, Saitama University, Saitama, Japan, H. Tajima Institute for Space-Earth Environmental Research, Nagoya University, Nagoya, Japan, M. Takahashi Institute for Cosmic Ray Research, University of Tokyo, Chiba, Japan, H. Takahashi Physics Program, Graduate School of Advanced Science and Engineering, Hiroshima University, Hiroshima, Japan, J. Takata Institute for Cosmic Ray Research, University of Tokyo, Chiba, Japan, R. Takeishi Institute for Cosmic Ray Research, University of Tokyo, Chiba, Japan, P. H. T. Tam Institute for Cosmic Ray Research, University of Tokyo, Chiba, Japan, S. J. Tanaka Department of Physical Sciences, Aoyama Gakuin University, Kanagawa, Japan, D. Tateishi Graduate School of Science and Engineering, Saitama University, Saitama, Japan, L. A. Tejedor IPARCOS-UCM, Instituto de Física de Partículas y del Cosmos, and EMFTEL Department, Universidad Complutense de Madrid, Madrid, Spain, P. Temnikov Institute for Nuclear Research and Nuclear Energy, Bulgarian Academy of Sciences, Sofia, Bulgaria, Y. Terada Graduate School of Science and Engineering, Saitama University, Saitama, Japan, K. Terauchi Division of Physics and Astronomy, Graduate School of Science, Kyoto University, Kyoto, Japan, T. Terzic University of Rijeka, Department of Physics, Rijeka, Croatia, M. Teshima Institute for Cosmic Ray Research, University of Tokyo, Chiba, Japan Max-Planck-Institut für Physik, München, Germany, M. Tluczykont Universität Hamburg, Institut für Experimentalphysik, Hamburg, Germany, F. Tokanai Department of Physics, Yamagata University, Yamagata, Yamagata, Japan, D. F. Torres Institute of Space Sciences, P. Travnicek FZU - Institute of Physics of the Czech Academy of Sciences, Praha, Czech Republic, S. Truzzi INFN and Università degli Studi di Siena, Dipartimento di Scienze Fisiche, della Terra e dell'Ambiente, A. Tutone INAF - Osservatorio Astronomico di Roma, Monteporzio Catone, Italy, G. Uhlrich University of Geneva - Département de physique nucléaire et corpusculaire, Genève, Switzerland, M. Vacula Palacky University Olomouc, Faculty of Science, Olomouc, Czech Republic, J. van Scherpenberg Max-Planck-Institut für Physik, München, Germany, M. Vázquez Acosta Instituto de Astrofísica de Canarias and Departamento de Astrofísica, Universidad de La Laguna, Tenerife, Spain, V. Verguilov Institute for Nuclear Research and Nuclear Energy, Bulgarian Academy of Sciences, Sofia, Bulgaria, I. Viale INFN Sezione di Padova and Università degli Studi di Padova, Padova, Italy, A. Vigliano INFN Sezione di Trieste and Università degli studi di Udine, Udine, Italy, C. F. Vigorito INFN Sezione di Torino, Torino, Italy Dipartimento di Fisica - Universitá degli Studi di Torino, Torino, Italy, V. Vitale INFN Sezione di Roma Tor Vergata, Rome, Italy, G. Voutsinas University of Geneva - Département de physique nucléaire et corpusculaire, Genève, Switzerland, I. Vovk Institute for Cosmic Ray Research, University of Tokyo, Chiba, Japan, T. Vuillaume Univ. Savoie Mont Blanc, CNRS, Laboratoire d'Annecy de Physique des Particules - IN2P3, Annecy, France, R. Walter Department of Astronomy, University of Geneva, Versoix, Switzerland, M. Will Max-Planck-Institut für Physik, München, Germany, T. Yamamoto Department of Physics, Konan University, Kobe, Hyogo, Japan, R. Yamazaki Department of Physical Sciences, Aoyama Gakuin University, Kanagawa, Japan, T. Yoshida Faculty of Science, Ibaraki University, Ibaraki, Japan, T. Yoshikoshi Institute for Cosmic Ray Research, University of Tokyo, Chiba, Japan, N. Zywucka Faculty of Physics and Applied Informatics, University of Lodz, Lodz, Poland, K. Bernloehr Max-Planck-Institut für Kernphysik, Heidelberg, Germany, O. Gueta Deutsches Elektronen-Synchrotron, Zeuthen, Germany, K. Kosack CEA/IRFU/SAp, CEA Saclay, Orme des Merisiers, Gif-sur-Yvette, France, G. Maier Deutsches Elektronen-Synchrotron, Zeuthen, Germany, J. Watson Deutsches Elektronen-Synchrotron, Zeuthen, Germany
Abstract: CTA (Cherenkov Telescope Array) is the next generation ground-based observatory for gamma-ray astronomy at very-high energies. The Large-Sized Telescope prototype (\LST{}) is located at the Northern site of CTA, on the Canary Island of La Palma. LSTs are designed to provide optimal performance in the lowest part of the energy range covered by CTA, down to $\simeq 20$ GeV. \LST{} started performing astronomical observations in November 2019, during its commissioning phase, and it has been taking data since then. We present the first \LST{} observations of the Crab Nebula, the standard candle of very-high energy gamma-ray astronomy, and use them, together with simulations, to assess the basic performance parameters of the telescope. The data sample consists of around 36 hours of observations at low zenith angles collected between November 2020 and March 2022. \LST{} has reached the expected performance during its commissioning period - only a minor adjustment of the preexisting simulations was needed to match the telescope behavior. The energy threshold at trigger level is estimated to be around 20 GeV, rising to $\simeq 30$ GeV after data analysis. Performance parameters depend strongly on energy, and on the strength of the gamma-ray selection cuts in the analysis: angular resolution ranges from 0.12 to 0.40 degrees, and energy resolution from 15 to 50\%. Flux sensitivity is around 1.1\% of the Crab Nebula flux above 250 GeV for a 50-h observation (12\% for 30 minutes). The spectral energy distribution (in the 0.03 - 30 TeV range) and the light curve obtained for the Crab Nebula agree with previous measurements, considering statistical and systematic uncertainties. A clear periodic signal is also detected from the pulsar at the center of the Nebula.
6.Slowly Rotating Accretion Flow Around SMBH in Elliptical Galaxy: Case With Outflow
Authors:Razieh Ranjbar, Shahram Abbassi
Abstract: Observational evidence and many numerical simulations show the existence of wind (i.e., uncollimated outflow) in accretion systems of the elliptical galaxy center. One of the primary aims of this study is to investigate the solutions of slowly rotating accretion flows around the supermassive black hole with outflow. This paper presents two distinct physical regions: supersonic and subsonic, that extend from the outer boundary to the black hole. In our numerical solution, the outer boundary is chosen beyond the Bondi radius. Due to strong gravity, we ignore outflow (i.e., $s = 0$) in the inner region (within $\sim 10 r_s$). The radial velocity of the flow at the outer region is significantly increased due to the presence of the outflow. Compared to previous works, the one accretion mode - namely, slowly rotating case, which corresponds to low accretion rates that have general wind output is carefully described, and the effect of galaxy potential and the feedback effects by the wind in this mode are taken into account. Since the power-law form of the mass accretion rate is mathematically compatible with our equations, we consider a radius-dependent mass accretion rate ($\dot{M}_{in} \propto r^s$), where $s$ is a free parameter and shows the intensity of outflow. There is an unknown mechanism for removing the mass, angular momentum, and energy by outflows in this study. The effects of the outflow appear well on the outer edge of the flow.